Elastic scattering and radiative capture of protons by C13

Hebbard, D.F.; Vogl, J. L.

doi:10.1016/0029-5582(60)90084-5

Cited by 66 publications

(75 citation statements)

References 24 publications

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“…[25]. In the first step, we performed a simultaneous fitting of the primary capture data of King et al [6] and the scattering data of Hebbard et al [9] without introducing any background poles. The ANCs were left as free parameters for χ 2 minimization and the ANCs resulted are listed in the fourth column of Table I.…”

Section: A Asymptotic Normalization Coefficientsmentioning

confidence: 99%

“…Data Set I consisted of the data of King, et al [6] for resonance R2, the data of Zeps, et al [15] for the ground state decay of resonance R5 and the elastic scattering data of Hebbard, et al [9] at θ lab = 90 o and 120 o . Data Set II, on the otherhand, comprised of the capture data of Genard et al [11] for the decay of R2 to the ground state of 14 N, the data of Zeps et al, the high energy tail part of the ground state decay of the resonance R2 from the data of King, et al [6] and the scattering data of Ref.…”

Section: B Simultaneous Fittingmentioning

confidence: 99%

“…The narrow d wave resonance of J π =2 − at excitation energy of 7.97 MeV does not have any significant contribution at energies of astrophysical interest. The capture reaction 13 C(p,γ) 14 N has been studied over a wide range of proton beam energies [6][7][8][9][10][11]. The cross section measurement was extended down to a beam energy of about 100 keV.…”

Section: Introductionmentioning

confidence: 99%

“…The cross section measurement was extended down to a beam energy of about 100 keV. Prior to the work of King et al [6], the measurements were restricted to the cross section for the decay to the ground state of 14 N [9,10]. Based on these data and with a correction of 18% [12] for cascade transitions, the recommended value of the astrophysical S-factor at zero energy was 5.5 keV.b [13].…”

Section: Introductionmentioning

confidence: 99%

“…[15]. The 13 C+p elastic scattering data of Hebbard, et al [9] over the centre of mass energy range of 200 to 700 keV at 90…”

Section: Introductionmentioning

confidence: 99%

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SystematicR-matrix analysis of theC13(p,γ)N
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deBoer
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et al. 2015
Phys. Rev. C
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Background: The proton capture reaction 13 C(p,γ) 14 N is an important reaction in the CNO cycle during the hydrogen burning in stars with mass greater than the mass of the Sun. It also occurs in the astrophysical sites like the red giant stars, the Asymptotic Giant Branch (AGB) stars. The low energy astrophysical S-factor of this reaction is dominated by a resonance state at an excitation energy of around 8.06 MeV (J π = 1 − ,T = 1) in 14 N. The other significant contributions come from the low energy tail of the broad resonance with J π = 0 − ,T = 1 at an excitation of 8.78 MeV and the direct capture process. Purpose: Measurements of low energy astrophysical S factor of the radiative capture reaction 13 C (p,γ) 14 N reported the extrapolated values of S(0) that differ by about 30%. Subsequent Rmatrix analysis and potential model calulations also yielded significantly different values for S(0). The present work intends to look into the dicrepancy through a detailed R-matrix analysis with emphasis on the associated uncertainties. Method A systematic reanalysis of the available decay data following the capture to the J π = 1 − , T = 1 resonance state of 14 N around 8.06 MeV excitation had been performed within the framework of R-matrix method. A simultaneous analysis of the 13 C(p,p0) data, measured over similar energy range, was carried out with the capture data. The data for the ground state decay of the broad resonance state (J π = 0 − , T = 1) around 8.78 MeV excitations was included as well. The external capture model along with the background poles to simulate the internal capture contribution were used to estimate the direct capture contribution. The asymptotic normalization constants (ANCs) for all states were extracted from the capture data. The multi-channel, multi-level R-matrix code AZURE2 was used for the calculation.Results The values of the astrophysical S-factor at zero relative energy, resulted from the present analysis are found to be consistent within the error bars for the two sets of capture data used. However, it is found from the fits to the elastic scattering data that the position of the J π = 1 − , T = 1 resonance state is uncertain by about 0.6 keV, prefering an excitation energy value of 8.062 MeV. Also the extracted ANC values for the states of 14 N corroborate with the values from the transfer reaction studies. The reaction rates from the present calculation are about 15-10 % lower than the values of NACRE II compilation but compares well with that from NACRE I. Conclusion The precise energy of the J π = 1 − , T = 1 resonance level around 8.06 MeV in 14 N must be determined. Further measurements around and below 100 keV with precision is necessary to reduce the uncertainty in the S-factor value at zero relative energy.

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Section: A Asymptotic Normalization Coefficientsmentioning

confidence: 99%